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Mitochondria are inherited maternally in most animals, but the mechanisms of selective paternal mitochondrial elimination (PME) are unknown. While examining fertilization in Caenorhabditis elegans, we observed that paternal mitochondria rapidly lose their inner membrane integrity. CPS-6, a mitochondrial endonuclease G, serves as a paternal mitochondrial factor that is critical for PME. We found that CPS-6 relocates from the intermembrane space of paternal mitochondria to the matrix after fertilization to degrade mitochondrial DNA. It acts with maternal autophagy and proteasome machineries to promote PME. Loss of cps-6 delays breakdown of mitochondrial inner membranes, autophagosome enclosure of paternal mitochondria, and PME. Delayed removal of paternal mitochondria causes increased embryonic lethality, demonstrating that PME is important for normal animal development. Thus, CPS-6 functions as a paternal mitochondrial degradation factor during animal development.

We demonstrate the feasibility of determining magnitudes of stars on archival photographic plates using a commercially available scanner. We describe one photometric approach that could serve as a useful example for other studies. In particular, we measure and calibrate stellar magnitudes from a 1903 photographic plate from the Yerkes Observatory collection, and demonstrate that the overall precision from our methods is better than 0.10 mag. Notably, these measurements are dominated by intrinsic plate noise, rather than noise introduced through the scanning/digitization process. The low expense of this approach expands the scientific potential to study variable stars in the archives of observatory plate collections. We use the serendipitous discovery of a candidate transient at photographic magnitude pg  = 16.60 in the spiral galaxy NGC 7331 to illustrate our photometric methods. If this unknown source is a supernova, it would represent the fourth known supernova in NGC 7331.

RNase T is a 3′-to-5′ exonuclease involved in RNA maturation pathways. Biochemical and three-dimensional structures of RNase T in complex with single- or double-stranded DNA reveal mechanisms of substrate selection and catalysis by this nuclease. RNA maturation relies on various exonucleases to remove nucleotides successively from the 5′ or 3′ end of nucleic acids. However, little is known regarding the molecular basis for substrate and cleavage preference of exonucleases. Our biochemical and structural analyses on RNase T–DNA complexes show that the RNase T dimer has an ideal architecture for binding a duplex with a short 3′ overhang to produce a digestion product of a duplex with a 2-nucleotide (nt) or 1-nt 3′ overhang, depending on the composition of the last base pair in the duplex. A 'C-filter' in RNase T screens out the nucleic acids with 3′-terminal cytosines for hydrolysis by inducing a disruptive conformational change at the active site. Our results reveal the general principles and the working mechanism for the final trimming step made by RNase T in the maturation of stable RNA and pave the way for the understanding of other DEDD family exonucleases.

We demonstrate the feasibility of determining magnitudes of stars on archival photographic plates using a commercially available scanner. We describe one photometric approach that could serve as a useful example for other studies. In particular, we measure and calibrate stellar magnitudes from a 1903 photographic plate from the Yerkes Observatory collection, and demonstrate that the overall precision from our methods is better than 0.10 mag. Notably, these measurements are dominated by intrinsic plate noise, rather than noise introduced through the scanning/digitization process. The low expense of this approach expands the scientific potential to study variable stars in the archives of observatory plate collections. We use the serendipitous discovery of a candidate transient at photographic magnitude pg = 16.60 in the spiral galaxy NGC 7331 to illustrate our photometric methods. If this unknown source is a supernova, it would represent the fourth known supernova in NGC 7331.

Six Sigma was developed by Motorola in the 1980s. While originally developed to improve manufacturing processes it has since been used by many organizations to improve all areas of business. Financial companies are starting to use Six Sigma in their businesses because they have found it to be profitable for them, but are these results industry wide? Are the companies currently using Six Sigma faring better than companies that do not? This paper intends to investigate the application of Six Sigma in financial services industry. [PUBLICATION ABSTRACT]

In the third paper from the COOL-LAMPS Collaboration, we report the discovery of COOL J0542-2125, a gravitationally lensed quasar at \\(z=1.84\\), observed as three images due to an intervening massive galaxy cluster at \\(z=0.61\\). The lensed quasar images were identified in a search for lens systems in recent public optical imaging data and have separations on the sky up to 25\".9, wider than any previously known lensed quasar. The galaxy cluster acting as a strong lens appears to be in the process of merging, with two sub-clusters separated by \\(\\sim 1\\) Mpc in the plane of the sky, and their central galaxies showing a radial velocity difference of \\(\\sim 1000\\) km/s. Both cluster cores show strongly lensed images of an assortment of background sources, as does the region between them. A preliminary strong lens model implies masses of \\(M(<250\\ \\rm{kpc}) = 1.79^{+0.16} _{-0.01} \\times 10^{14} M_{\\odot}\\) and \\(M(<250\\ \\rm{kpc}) = 1.48^{+0.04}_{-0.10} \\times 10^{14} M_{\\odot}\\) for the East and West sub-clusters, respectively. This line of sight is also coincident with a ROSAT ALL-sky Survey source, centered between the two confirmed cluster halos reminiscent of other major cluster-scale mergers.

We demonstrate the feasibility of determining magnitudes of stars on archival photographic plates using a commercially available scanner. We describe one photometric approach that could serve as a useful example for other studies. In particular, we measure and calibrate stellar magnitudes from a 1903 photographic plate from the Yerkes Observatory collection, and demonstrate that the overall precision from our methods is better than 0.10 mag. Notably, these measurements are dominated by intrinsic plate noise, rather than noise introduced through the scanning/digitization process. The low expense of this approach expands the scientific potential to study variable stars in the archives of observatory plate collections. We use the serendipitous discovery of a candidate transient at photographic magnitude \\(pg\\) = 16.60 in the spiral galaxy NGC 7331 to illustrate our photometric methods. If this unknown source is a supernova, it would represent the fourth known supernova in NGC 7331.

We present COOL J1323+0343, an early-type galaxy at \\(z = 1.0153 \\pm 0.0006\\), strongly lensed by a cluster of galaxies at z = \\(z = 0.353 \\pm 0.001\\). This object was originally imaged by DECaLS and noted as a gravitational lens by COOL-LAMPS, a collaboration initiated to find strong-lensing systems in recent public optical imaging data, and confirmed with follow-up data. With ground-based grzH imaging and optical spectroscopy from the Las Campanas Observatory and the Nordic Optical Telescope, we derive a stellar mass, metallicity, and star-formation history from stellar-population synthesis modeling. The lens modeling implies a total magnification of \\(\\mu \\sim \\)113. The median remnant stellar mass in the source plane is M\\(_* \\sim 10.63\\) \\(M_\\odot\\) and the median star-formation rate in the source plane is SFR \\(\\sim 1.55 \\times 10^{-3}\\) M\\(_\\odot\\) yr\\(^{-1}\\) (log sSFR = -13.4 yr\\(^{-1}\\)) in the youngest two age bins (0-100 Myr), closest to the epoch of observation. Our measurements place COOL J1323+0343 below the characteristic mass of the stellar mass function, making it an especially compelling target that could help clarify how intermediate mass quiescent galaxies evolve. We reconstruct COOL J1323+0343 in the source plane and fit its light profile. This object is below the expected size-evolution of early-type galaxy at this mass with an effective radius r\\(_e \\sim\\) 0.5 kpc. This extraordinarily magnified and bright lensed early-type galaxy offers an exciting opportunity to study the morphology and star formation history of an intermediate mass early-type galaxy in detail at \\(z \\sim \\)1 .

We report the discovery of COOL J1241+2219, a strongly-lensed galaxy at redshift \\(z\\)=5.043\\(\\pm\\)0.002 with observed magnitude \\(z_{AB}=20.47\\), lensed by a moderate-mass galaxy cluster at \\(z\\)=1.001\\(\\pm\\)0.001. COOL J1241+2219 is the brightest lensed galaxy currently known at optical and near-infrared wavelengths at \\(z\\) \\(\\gtrsim\\) 5; it is \\(\\sim\\)5 times brighter than the prior record-holder lensed galaxy, and several magnitudes brighter than the brightest unlensed galaxies known at these redshifts. It was discovered as part of COOL-LAMPS, a collaboration initiated to find strongly lensed systems in recent public optical imaging data. We characterise the lensed galaxy, as well as the central galaxy of the lensing cluster using ground-based \\(griz\\)JH imaging and optical spectroscopy. We report model-based magnitudes, and derive stellar masses, dust content, metallicity and star-formation rates via stellar-population synthesis modeling. Our lens mass modeling, based on ground-based imaging, implies a median source magnification of \\(\\sim\\)30, which puts the stellar mass and star formation rate (in the youngest age bin, closest to the epoch of observation) at logM\\(_{*}\\) = \\(10.11^{+0.21}_{-0.26}\\) and SFR = \\(27^{+13}_{-9}\\) M\\(_{\\odot}\\)/yr, respectively. We constrain a star formation history for COOL J1241+2219 consistent with constant star formation across \\(\\sim\\)1 Gyr of cosmic time, and that places this galaxy on the high-mass end of the star-forming main sequence. COOL J1241+2219 is 2-4 times more luminous than a galaxy with the characteristic UV luminosity at these redshifts. The UV continuum slope \\(\\beta\\)= -2.2\\(\\pm\\)0.2 places this galaxy on the blue side of the observed distribution of galaxies at \\(z\\)=5, although the lack of Ly\\(\\alpha\\) emission indicates dust sufficient to suppress this emission.